In the following, we show the results of numerical calculations of the
equations described above. The linear power spectrum \(P_\mathrm {L}(k)\) 
of the mass density is calculated by a Boltzmann code CLASS
[1]}, [2]} with a flat \(\Lambda \) CDM model
and cosmological parameters \(h=0.6732\) ,
\(\Omega _{\mathrm {b}0}h^2=0.02238\) , \(\Omega _{\mathrm {cdm}}h^2=0.1201\) ,
\(n_\mathrm {s}=0.9660\) , \(\sigma _8=0.8120\)  (Planck 2018
[3]}). We apply a smoothing radius of
\(R=5\,h^{-1}\mathrm {Mpc}\)  in the smoothing function of the biasing
model. All the bias parameters are simply substituted by unity,
\(b^{(1)}_{X2} = b^{(2)}_{X2.00} = b^{(2)}_{X2;02} = b^{(2)}_{X2;20} =b^{(2)}_{X2;22} = 1\) . The interchange symmetry of
Eq. (REF ) requires an indentity,
\(b^{(2)}_{X2;02} = b^{(2)}_{X2;20}\) . For the fast Hankel transforms,
we use a Mathematica version of the numerical
codehttps://jila.colorado.edu/ ajsh/FFTLog/ FFTLog
[4]}.
